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A numerical detection of the $\tau$-driven transition of galaxy spins ispresented, where $\tau$ is the degree of misalignment between the initial tidalfield and protogalaxy inertia tensors. Analyzing the data from the IllustrisTNG300-1 simulations, we first measure the values of $\tau$ at the protogalacticsites found by tracing the constituents of the galactic halos in the mass rangeof $10.5\le \log \left[M_{h}/(h^{-1}M_{\odot})\right] \le 13$ back to theinitial stage, $z_{i}=127$. The probability density functions of $\tau$ areshown to be well modeled by the $\Gamma$-distributions, whose shape and scaleparameters turn out to have universal values on a certain critical scale. Then,we investigate how the strength and tendency of the galaxy spin alignments withthe principal axes of the local tidal fields depend on the initial condition,$\tau$. It is found that on the scale lower than the critical one, the galaxyspin transition occurs at two different thresholds from the major tointermediate and from the intermediate to minor principal axes of the localtidal fields, respectively. Noting that the $\tau$-dependent spin transitionsupersedes in strength the previously found mass-dependent,morphology-dependent, and radius-dependent counterparts, we suggest that $\tau$should be the key driver of all types of the galaxy spin transition and thatthe present galaxy spins are indeed excellent fossil records of the initialcondition.

Galaxy Spin Transition Driven by the Misalignments between the Protogalaxy Inertia and Initial Tidal Tensors